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5741. http://hea-www.harvard.edu/AstroStat/SolStat2012/jack_ireland.pdf
... Solar structures oscillate Ї Ї many different oscillation periods have been identified - lots of frequency space to examine. concentrate on 3 and 5 minute wavebands. ... Identification of oscillating individual pixels, then segmentation into significant groups Data Ї Ї Ї Ї Use SPoCA active region detections. ... Analysis Ї Ї Oscillation model in each pixel dj = A cos( tj )+ B sin( tj ) Calculate (Bayesian) probability p() that the timeseries dj observed at times tj= j.t (1jN) supports a frequency . ...
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Ссылки http://hea-www.harvard.edu/AstroStat/SolStat2012/jack_ireland.pdf -- 284.9 Кб -- 22.06.2012
[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/SolStat2012/jack_ireland.pdf -- 284.9 Кб -- 22.06.2012
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[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/SolStat2012/jack_ireland.pdf -- 284.9 Кб -- 22.06.2012
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5742. http://hea-www.harvard.edu/hea/section_image.inc
<!-- SectionPhoto --><br> <img src="/common/images/left_ressci.jpg" alt="Section Photo" width="156" height="214">
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Ссылки http://hea-www.harvard.edu/hea/section_image.inc -- 1.1 Кб -- 21.06.2012
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5743. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/modfits.py
Jaesub Hong, Nov, 2011 # # append lines or rows to a fits table # the data structure of the table is manually handled. # # an example usage --------------------------- ... import struct as st # fits=mf.modfits( this.fits ) # open the fits file # fits.rewind(50) # start from the last 50th lines # for i in range(100): # add 100 lines # fits.append( gz%5d % i + st.pack(' fffff',0.0,0.1,1.1e2,2.2e3,3.3e4) ) # fits.close(1) # close the file # # --- ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/modfits.py -- 4.0 Кб -- 12.06.2012
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5744. http://hea-www.harvard.edu/~saku/cvplus.pdf
... 2010 Suzaku X-ray Spectra and Pulse Profile Variations during the Superorbital Cycle of LMC X-4 (L. Hung, R. Hickox, B.S. Boroson, & S.D. Vrtilek), ApJ, 720, 1202. 2010 X-ray Variations at the Orbital Period from Cygnus X-1 in the High/Soft State (B.S. Boroson, & S.D. Vrtilek), ApJ, 710, 197. ... 2008 Ultraviolet Observations of the X-ray Photoionized Wind of Cygnus X-1 during X-ray Soft/High State (S.D. Vrtilek, B. Boroson, A. Hunacek, D. Geis, & C.T. Bolton), ApJ, 678, 1248. ... ApJ, 555, 477. ...
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Ссылки http://hea-www.harvard.edu/~saku/cvplus.pdf -- 75.7 Кб -- 11.06.2012
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5745. http://hea-www.harvard.edu/~saku/cvplus.ps
... 2010 Suzaku Xґray Spectra and Pulse Profile Variations during the Superorbital Cycle of LMC Xґ4 (L. Hung, R. Hickox, B.S. Boroson, & S.D. Vrtilek), ApJ, 720, 1202. ... 2008 Ultraviolet Observations of the Xґray Photoionized Wind of Cygnus Xґ1 during Xґray Soft/High State (S.D. Vrtilek, B. Boroson, A. Hunacek, D. Geis, & C.T. Bolton), ApJ, 678, 1248. ... 2001 The Chandra View of Xґray Binaries (S.D. Vrtilek) in High Energy Uniґ verse at Sharp Focus: Chandra Science ASP Conference Proceedings Vol. ...
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Ссылки http://hea-www.harvard.edu/~saku/cvplus.ps -- 131.7 Кб -- 11.06.2012
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5746. http://hea-www.harvard.edu/ChaMPlane/papers/1203-draft-jaesub-grxe.pdf
... Recently Revnivtsev et al (2009) (R09) claimed that 90% of the 6.5ґ7.1 keV X-ray flux from a small section of a low extinction region at 1.4 south of the Galactic Center has been resolved to discrete sources with LX, 2-10 keV 4в10-16 erg s-1 cm-2 , using ultra-deep (1 Ms) Chandra ACIS-I observations. ... R09 used a fixed 2 radius circle around each source for the source aperture and the rest of the HRES region (excluding all the source regions) for the background region. ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/papers/1203-draft-jaesub-grxe.pdf -- 1536.4 Кб -- 01.06.2012
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5747. http://hea-www.harvard.edu/~kim/pap/2012_YoungE_ISM_published.pdf
... In two young elliptical galaxies (NGC 720 and NGC 3923) we find that the Si to Fe abundance ratio is super-solar (at a 99% significance level), in contrast to typical old elliptical galaxies where the Si to Fe abundance ratio is close to solar. ... Comparison of the abundance ratios (in solar unit) measured with Xray spectra extracted from the central regions (r < 30 ) of two young elliptical galaxies and six old elliptical galaxies. ... The O to Fe ratio is 0.3 solar in NGC 5044 (Buote et al. ...
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Ссылки http://hea-www.harvard.edu/~kim/pap/2012_YoungE_ISM_published.pdf -- 875.1 Кб -- 03.05.2012
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5748. http://hea-www.harvard.edu/~saku/modmapcookbookmod.pdf
... MEM iterations S .. ... empty]test.mol Rest wavelength:[0= 6562.76] 6562.76 MOLLY File opened : test.mol Error reading MOLLY headers 43 spectra read. ... If unknown, use your best guess for (radial velocity ); you can check this using different values in modmap . (250 pixels at 0.8angstroms/pixel; better to oversample) modmap v Rest wavelength (A) : 6562.75788 Gamma velocity : -44 Number of pixels in velocity grid : 100 Maximum velocity in tomogram: 2000 FWHM of local line profile: 100 ...
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Ссылки http://hea-www.harvard.edu/~saku/modmapcookbookmod.pdf -- 77.8 Кб -- 10.04.2012
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5749. http://hea-www.harvard.edu/~saku/MollyInstructionsmod.pdf
... Opened1: /data.saku/software/F77/molly/startup Maximum spectrum length set = 4000 Maximum number of spectra = 7500 Files will be written even if a file of the same name exists. ... Quit Assign the data Enter the data file name Open files for editing 1]: 1 1]: 2 (Where 1 2 are the first and last file numbers to edit) edit file Enter filename [header]: molly .info Variable Variable Variable Variable Variable Variable Variable Variable Variable edit Quit 1 2 3 4 5 6 7 8 9 name: name ...
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Ссылки http://hea-www.harvard.edu/~saku/MollyInstructionsmod.pdf -- 91.0 Кб -- 10.04.2012
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5750. http://hea-www.harvard.edu/~saku/dopplerinstructions.pdf
... The process consists of creating a starting image, scaling it to the optimal starting image for the data, then iterating it with the data to produce a tomogram. ... Depending on where the line in questions is being emitted, it may help to start with a Gaussian instead of a flat image, by setting 'fancy' to 'TRUE', but in most cases a flat image works equally well. If you are creating tomograms for lines which are blended or very close, you may need to set the number of images and lines higher. ...
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Ссылки http://hea-www.harvard.edu/~saku/dopplerinstructions.pdf -- 65.9 Кб -- 10.04.2012
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5751. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/strreplace.pro
NAME: ; STRREPLACE ; ; PURPOSE: ; The STRREPLACE procedure replaces the contents of one string ; with another. The first occurrence of the search substring, Find ; within the source string, String is replaced by the string, ; Replacement. ... CALLING SEQUENCE: ; ; STRREPLACE, String, Find, Replacement ; ; INPUTS: ; String: The string to have substring(s) replaced. ... Find: The scalar substring to be replaced. ... Replacement: A scalar string to replace the Find substring. ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/strreplace.pro -- 3.2 Кб -- 20.03.2012
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5752. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/rdrdb2.pro
JaeSub Hong, 2002-2005, version 1.5 ; Please report any problem or suggestion at jaesub@head.cfa.harvard.edu ; ; ; - consider any line starting with # comments ; - speed up by pre-setting array size (default 1000, change by n_step) ; function rdrdb2, filename, $ noheader=noheader, comment = comment , $ data = data , sep = sep , struct = struct , recycle=recycle, $ names = names , units=units, n_step=n_step, n_ data =n_ ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/rdrdb2.pro -- 4.3 Кб -- 20.03.2012
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5753. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/readme.txt
grid.py : python program to generate grid files uses sherpa under ciao ver 4.3 e.g. this will generate a grid file in the fits format ( output.qgrid.fits ) and sherpa script used to calculate grid for reference ( sherpa _ grid .sph). grid.py \ --rmf=example.rmf \ --arf=example.arf \ -- fits = output.qgrid.fits \ --model= xsphabs.A*xspowerlaw.B \ --par1=A.nH: 0.01 , ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/readme.txt -- 1.6 Кб -- 19.03.2012
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5754. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/example.pro
.r qdplot2 fgrid='output.qgrid.fits' xr=[0.1,1.0] yr=[0.0,3.0] xtit='' qd_plot2, range=[0.3,8.0], $ xr=xr, yr=yr, $ grid=grid, $ col=[60,150], $ file_grid=fgrid, $ xtit=xtit, $ type='pl2'
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/example.pro -- 1.2 Кб -- 19.03.2012
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5755. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/grid.py
usr/bin/env python # global script for automation # this is for sherpa in ciao 4.3 # examples # grid.py \ # -- rmf =example. rmf \ # -- arf =example. arf \ # --fits=output.qgrid.fits \ # -- model = xsphabs.A*xspowerlaw.B \ # -- par1 =A.nH:0.01,0.1,0.4,1,4,10:200 \ # -- par2 =B.PhoIndex:0,1,2,3,4:200 \ # -- etcp =B.norm:1.0 # --range=0.3,8.0 import subprocess as sp import sys import re import numpy from time import time, localtime #from scipy ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/grid.py -- 9.5 Кб -- 19.03.2012
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5756. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/qdplot2.pro
J.E. Grindlay, ; 2004 ApJ 614 p508 and references therein ; ; quantile diagram plotting routine ; now with fits format for grid files ; and the default x axis is log of median ; require rdrdb.pro (included) ;======================================================================== pro qd_setwin, xr=xr, yr=yr, $ xtit=xtit,ytit=ytit, $ xty=xty,yty=yty, $ xtick=xt, range = range , xtv=xtv, $ noxtick=noxtick, noytick=noytick, $ noxtoptick=noxtoptick, $ stu=stu, noerase=noerase, ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/qdplot2.pro -- 25.8 Кб -- 19.03.2012
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5757. http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/sherpa_grid.sph
interpolate as interpol import numpy as np frac=[0.25,0.5,0.75] set_source( faked , xsphabs.A*xspowerlaw.B ) par1s = [0.01,0.1,0.4,1,4,10] par2s = [0,1,2,3,4] B.norm=1.0 cpar1s = [] npar1s = len( par1s ) for ii in range(0, npar1s-1): for par in np.arange( par1s [ii], par1s [ii+1],1.*npar1s*( par1s [ii+1]- par1s [ii])/200): cpar1s.append(par) cpar2s = [] npar2s = len( par2s ) for ii in range(0, npar2s-1): for par in np.arange( ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/quantile/4ciao4.3/sherpa_grid.sph -- 3.9 Кб -- 19.03.2012
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5758. http://hea-www.harvard.edu/AstroStat/Stat310_1112/ICASSP12_SDWH.pdf
POISSON NOISE REDUCTION WITH NON-LOCAL PCA J. Salmon C-A. Deledalle R. Willett Z. Harmany Duke University, ECE Department Durham, NC, USA CEREMADE, CNRS-Paris-Dauphine, Paris, France the data, a point of view also adopted in [13]. ... We apply patch based methods (also referred to as Non-Local methods) to Poisson noise, adapting PCA-based denoising in this heteroscedastic context. ... We coined our method Poisson NL-PCA, (for Non-Local Principal Component Analysi). ...
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Ссылки http://hea-www.harvard.edu/AstroStat/Stat310_1112/ICASSP12_SDWH.pdf -- 633.4 Кб -- 10.03.2012
[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/Stat310_1112/ICASSP12_SDWH.pdf -- 633.4 Кб -- 10.03.2012
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[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/Stat310_1112/ICASSP12_SDWH.pdf -- 633.4 Кб -- 10.03.2012
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5759. http://hea-www.harvard.edu/AstroStat/SolStat2012/ePoster_dstenning.pdf
... X CB (X) Opening of a set X by a disk B. Closing of a set X by a disk B. Science-Driven Feature Selection (a) (b) Mount Wilson Classification The Mount Wilson classification scheme groups sunspots into four classes based on the complexity of magnetic flux distribution in associated active regions [1]: class : groups dominated by a single unipolar sunspot class : a pair of sunspots of opposite magnetic ... Convex hulls are utilized to measure polarity mixture in (j). ...
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Ссылки http://hea-www.harvard.edu/AstroStat/SolStat2012/ePoster_dstenning.pdf -- 406.1 Кб -- 01.03.2012
[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/SolStat2012/ePoster_dstenning.pdf -- 406.1 Кб -- 01.03.2012
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[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/SolStat2012/ePoster_dstenning.pdf -- 406.1 Кб -- 01.03.2012
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5760. http://hea-www.harvard.edu/AstroStat/SolStat2012/eposter_jpossonbrown.pdf
... Thursday, February 16, 2012 Goal Event detection in presence of variable background (e.g. Figure 1), without Event Detection Codes knowledge of background. ... Thursday, February 16, 2012 Simulate lightcurves to test codes Figure 2 Simulated lightcurve with 64 events added to a constant background. ... Thursday, February 16, 2012 Calibrate false positives w/ zero event LCs Figure 3 Calibrating the event detection algorithms to optimize false positives, using the simulated lightcurves with zero...
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Ссылки http://hea-www.harvard.edu/AstroStat/SolStat2012/eposter_jpossonbrown.pdf -- 897.2 Кб -- 22.02.2012
[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/SolStat2012/eposter_jpossonbrown.pdf -- 897.2 Кб -- 22.02.2012
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[ Текст ] Ссылки http://hea-www.harvard.edu/astrostat/SolStat2012/eposter_jpossonbrown.pdf -- 897.2 Кб -- 22.02.2012
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